Show simple item record

dc.contributor.authorPallottini, Andreaen
dc.contributor.authorFerrara, Aen
dc.contributor.authorGallerani, Sen
dc.contributor.authorVallini, Len
dc.contributor.authorMaiolino, Robertoen
dc.contributor.authorSalvadori, Sen
dc.date.accessioned2017-01-27T12:07:29Z
dc.date.available2017-01-27T12:07:29Z
dc.date.issued2017-03-01en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/262085
dc.description.abstractWe present zoom-in, AMR, high-resolution ($\simeq 30$ pc) simulations of high-redshift ($z \simeq 6$) galaxies with the aim of characterizing their internal properties and interstellar medium. Among other features, we adopt a star formation model based on a physically-sound molecular hydrogen prescription, and introduce a novel scheme for supernova feedback, stellar winds and dust-mediated radiation pressure. In the zoom-in simulation the target halo hosts "Dahlia", a galaxy with a stellar mass $M_*=1.6\times 10^{10}$M$_\odot$, representative of a typical $z\sim 6$ Lyman Break Galaxy. Dahlia has a total H2 mass of $10^{8.5}$M$_\odot$, that is mainly concentrated in a disk-like structure of effective radius $\simeq 0.6$ kpc and scale height $\simeq 200$ pc. Frequent mergers drive fresh gas towards the center of the disk, sustaining a star formation rate per unit area of $\simeq 15 $M$_\odot$ yr$^{-1}$ kpc$^{-2}$. The disk is composed by dense ($n \gtrsim 25$ cm$^{-3}$), metal-rich ($Z \simeq 0.5 $ Z$_\odot$) gas, that is pressure-supported by radiation. We compute the $158\mu$m [CII] emission arising from Dahlia, and find that $\simeq 95\%$ of the total [CII] luminosity ($L_{[CII]}\simeq10^{7.5}$ L$_\odot$) arises from the H2 disk. Although $30\%$ of the CII mass is transported out of the disk by outflows, such gas negligibly contributes to [CII] emission, due to its low density ($n \lesssim 10$ cm$^{-3}$) and metallicity ($Z\lesssim 10^{-1}$Z$_\odot$). Dahlia is under-luminous with respect to the local [CII]-SFR relation; however, its luminosity is consistent with upper limits derived for most $z\sim6$ galaxies.
dc.description.sponsorshipThis research was supported in part by the National Science Foundation under Grant No. NSF PHY11-25915. SS was supported by the European Research Council through a Marie–Skodolowska–Curie Fellowship, project PRIMORDIAL-700907. RM acknowledges support from the ERC Advanced Grant 695671 ‘QUENCH’ and from the Science and Technology Facilities Council (STFC).
dc.language.isoenen
dc.publisherOxford University Press
dc.subjectmethods: numericalen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: formationen
dc.subjectgalaxies: highredshiften
dc.subjectgalaxies: ISMen
dc.subjectinfrared: generalen
dc.titleZooming on the internal structure of $z\simeq6$ galaxiesen
dc.typeArticle
prism.endingPage2558
prism.issueIdentifier3en
prism.publicationDate2017en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage2540
prism.volume465en
dc.identifier.doi10.17863/CAM.7333
dcterms.dateAccepted2016-11-02en
rioxxterms.versionofrecord10.1093/mnras/stw2847en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2017-03-01en
dc.contributor.orcidPallottini, Andrea [0000-0002-7129-5761]
dc.contributor.orcidMaiolino, Roberto [0000-0002-4985-3819]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSTFC (ST/K003119/1)
pubs.funder-project-idSTFC (ST/M001172/1)
pubs.funder-project-idECH2020 EUROPEAN RESEARCH COUNCIL (ERC) (695671)
cam.issuedOnline2016-11-04en
cam.orpheus.successThu Jan 30 12:56:43 GMT 2020 - The item has an open VoR version.*
rioxxterms.freetoread.startdate2100-01-01


Files in this item

Thumbnail
Thumbnail

This item appears in the following Collection(s)

Show simple item record